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We use a high-resolution simulation of a galaxy-sized dark matter halo, published simulated data as well as four cluster-sized haloes from Fukushige, Kawai & Makino (2003) to study the inner halo structure in a ΛCDM cosmology. We find that the circular velocity

We use a high-resolution simulation of a galaxy-sized dark matter halo, published simulated data as well as four cluster-sized haloes from Fukushige, Kawai & Makino (2003) to study the inner halo structure in a ΛCDM cosmology. We find that the circular velocity Minimize

One of the greatest challenges to the Λ cold dark matter (CDM) model favoured today is probably the apparent discrepancy between the very inner parts of observed dark matter (DM) density profiles and their counterparts in cosmological N-body simulations

One of the greatest challenges to the Λ cold dark matter (CDM) model favoured today is probably the apparent discrepancy between the very inner parts of observed dark matter (DM) density profiles and their counterparts in cosmological N-body simulations Minimize

In hierarchical cosmologies such as the now-standard ΛCDM model, objects like the dark halo of our Milky Way are built up through the merger and accretion of previously collapsed systems with a very wide range of masses. Even the earliest

In hierarchical cosmologies such as the now-standard ΛCDM model, objects like the dark halo of our Milky Way are built up through the merger and accretion of previously collapsed systems with a very wide range of masses. Even the earliest Minimize

We present a semi–analytic treatment of galactic winds within high resolution, large scale cosmological N–body simulations of a ΛCDM Universe. The evolution of winds is investigated by following the expansion of supernova driven supershells around the several hundred thousand galaxies that form in an approximately spherical region of space with ...

We present a semi–analytic treatment of galactic winds within high resolution, large scale cosmological N–body simulations of a ΛCDM Universe. The evolution of winds is investigated by following the expansion of supernova driven supershells around the several hundred thousand galaxies that form in an approximately spherical region of space with diameter 52h −1 Mpc and mean density close to the mean density of the Universe. We focus our attention on the impact of winds on the diffuse intergalactic medium. Initial conditions for mass loss at the base of winds are taken from Shu, Mo & Mao (2003). Results are presented for the volume filling factor and the mass fraction of IGM in winds and their dependence on the model parameters is carefully investigated. We find that a high volume filling factor does not necessarily correspond to a high mass fraction in wind shells, implying that even very spatially extended galactic winds may not leave detectable imprints on the Lyα forest. Low mass galaxies play a major role in seeding the IGM with metals at high redshift in models where winds sweep up little gas from the IGM and supernova ejecta constitute most of the mass in shells. The formation of winds in low mass galaxies is instead suppressed in models in which the mass of IGM entrained in winds is significant. In these models, the IGM is enriched at later times by galaxies with large stellar masses. Minimize

We compare the structure and kinematics of the 11 known satellites of the Milky Way with high resolution simulations of the formation of its dark halo in a ΛCDM universe. In contrast to earlier work, we find excellent agreement. The observed kinematics are

We compare the structure and kinematics of the 11 known satellites of the Milky Way with high resolution simulations of the formation of its dark halo in a ΛCDM universe. In contrast to earlier work, we find excellent agreement. The observed kinematics are Minimize

The dwarf satellite galaxies of the Milky Way are the most dark matter dominated systems known to date in the Universe. They represent a heterogeneous population in terms of their stellar properties

The dwarf satellite galaxies of the Milky Way are the most dark matter dominated systems known to date in the Universe. They represent a heterogeneous population in terms of their stellar properties Minimize

We have extended the Tiny Tim HST point-spread function simulator so that it can now generate PSFs for the Wide Field Camera 3. This ISR describes the changes and sources of information used and shows some comparisons between modeled PSFs and those observed with the CASTLE stimulus during thermal vacuum testing. A web interface to the same simul...

We have extended the Tiny Tim HST point-spread function simulator so that it can now generate PSFs for the Wide Field Camera 3. This ISR describes the changes and sources of information used and shows some comparisons between modeled PSFs and those observed with the CASTLE stimulus during thermal vacuum testing. A web interface to the same simulation software is also available. Minimize